NGC 2427

Last updated
NGC 2427
NGC 2427 hst 09042 31 R814GB450.png
NGC 2427 imaged by the Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Puppis
Right ascension 07h 36m 28.035s [1]
Declination −47° 38′ 11.05″ [1]
Redshift 0.003242 ± 0.000010 [1]
Heliocentric radial velocity 972 ± 3 km/s [1]
Distance 35.3 ± 4.8 Mly (10.8 ± 1.5 Mpc) [1]
Apparent magnitude  (V)11.6 [2]
Characteristics
Type SAB(s)c pec [1]
Size~53,000  ly (16.3  kpc) (estimated) [1]
Apparent size  (V)5.2′ × 2.2′ [1]
Other designations
ESO 208- G 027, IRAS 07350-4731, PGC 21375 [1]

NGC 2427 is a barred spiral galaxy located in the constellation Puppis. It is located at a distance of about 35 million light years from Earth, which, given its apparent dimensions, means that NGC 2427 is about 50,000 light years across. [1] It was discovered by John Herschel on March 1, 1835. [3]

Contents

NGC 2427 has a bright short bar and two main spiral arms. The arms are asymmetric and of low surface brightness and feature many knots and HII regions the largest of which are about one arcsecond across. [4] [5] [6] The total star formation rate is estimated to be 1.1 M☉ per year. [7] When observed in H-alpha the bar is well defined and narrow and appears about one arcminute long across the galactic bulge. Many faint HII regions are visible in the inner and extended eastern disk of the galaxy. As the galaxy lies near the galactic plane and is seen in high inclination it is difficult to trace the spiral arms in H-alpha. [8] The nucleus is very small and faint [5] and hosts a nuclear star cluster which is 3.2 arcseconds across. [9]

NGC 2427 is a member of a galaxy group which also includes the galaxies NGC 2502, ESO 208- G 021, and ESO 209- G 009. [10]

See also

References

  1. 1 2 3 4 5 6 7 8 9 10 "NASA/IPAC Extragalactic Database". Results for NGC 2427. Retrieved 2016-01-18.
  2. ↑ "Revised NGC Data for NGC 2427". spider.seds.org. Retrieved 25 November 2018.
  3. ↑ Seligman, Courtney. "NGC 2427". Celestial Atlas. Retrieved 19 November 2018.
  4. ↑ Corwin, H. G.; de Vaucouleurs, A.; de Vaucouleurs, G (1985) Southern Galaxy Catalogue. University of Texas
  5. 1 2 de Vaucouleurs, Gerard Henri; de Vaucouleurs, Antoinette; Shapley, Harlow (1964). Reference catalogue of bright galaxies. Austin: University of Texas Press. Bibcode:1964rcbg.book.....D.
  6. ↑ Sandage, A.; Brucato, R. (April 1979). "The Las Campanas survey of bright southern galaxies. II - New classifications for 153 systems". The Astronomical Journal. 84: 472. Bibcode:1979AJ.....84..472S. doi:10.1086/112440.
  7. ↑ Parkash, Vaishali; Brown, Michael J. I.; Jarrett, T. H.; Bonne, Nicolas J. (1 September 2018). "Relationships between Hi Gas Mass, Stellar Mass, and the Star Formation Rate of HICAT+WISE (H i-WISE) Galaxies". The Astrophysical Journal. 864 (1): 40. Bibcode:2018ApJ...864...40P. doi: 10.3847/1538-4357/aad3b9 .
  8. ↑ Ryder, Stuart D.; Dopita, Michael A. (October 1993). "An H-alpha atlas of nearby southern spiral galaxies". The Astrophysical Journal Supplement Series. 88: 415. Bibcode:1993ApJS...88..415R. doi:10.1086/191827.
  9. ↑ Georgiev, Iskren Y.; Böker, Torsten; Leigh, Nathan; Lützgendorf, Nora; Neumayer, Nadine (1 April 2016). "Masses and scaling relations for nuclear star clusters, and their co-existence with central black holes". Monthly Notices of the Royal Astronomical Society. 457 (2): 2122–2138. doi: 10.1093/mnras/stw093 .
  10. ↑ Crook, Aidan C.; Huchra, John P.; Martimbeau, Nathalie; Masters, Karen L.; Jarrett, Tom; Macri, Lucas M. (February 2007). "Groups of Galaxies in the Two Micron All Sky Redshift Survey". The Astrophysical Journal. 655 (2): 790–813. arXiv: astro-ph/0610732 . Bibcode:2007ApJ...655..790C. doi:10.1086/510201.
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